Einstein Observations of the SNRs IC443, W44 and W49B

Watson, M. G.; Willingale, R.; Pye, J. P.; Rolf, Daniel; Wood, Norman B.; Thomas, N.; Seward, F. D.

doi:10.1007/978-94-009-7231-5_39

Cited by 4 publications

(3 citation statements)

References 12 publications

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“…Figure 2 Nevertheless their total contribution is definitely less than the height of peaks in the contours. The superposition in Figure 1 shows that the leading edge of optical filaments and the edge of the [Fex] emission coincide fairly well, in agreement with the less-resolved data of WLS and with the X-ray data (e.g., Petre et al 1983;Watson et al 1983). We also see what appears to be a surface brightness gradient running from the southeastern to the northwestern corners of Figure 1, again in Fig.…”

Section: Observationssupporting

confidence: 81%

“…There is a consensus that the shock front of the supernova remnant IC 443 is colliding with a cold molecular cloud. The interaction is probably simultaneously responsible for the cold shocked gas observed at 21 cm (Giovanelli and Haynes 1979), the bright optical filaments in the NE portion, and the X-rays emitted from much of the region (e.g., Petre et al 1983;Watson et al 1983). The spectral energy distribution at X-ray wavelengths is thermal and characterized by logT near 7.0, and may be explained by a Sedov blast-wave model (Winkler and Clark 1974;Malina, Bowyer, and Lampton 1979), indicating that the remnant is probably in its adiabatic, middleaged phase.…”

Section: Introductionmentioning

confidence: 99%

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An observation of IC 443 in the forbidden coronal lambda 6374 line

Gensheimer¹,

Teske²

1986

PASP

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Section: Observationssupporting

confidence: 81%

Section: Introductionmentioning

confidence: 99%

An observation of IC 443 in the forbidden coronal lambda 6374 line

Gensheimer¹,

Teske²

1986

PASP

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“…The centrally peaked X-ray morphology was first noted in observations from the Einstein Observatory Image Proportional Counter (IPC; Watson et al 1983;Smith et al 1985). Assuming the X-ray emission to be thermal (Szymkowiak 1980;Jones et al 1993), the morphology of the emission was explained by a scenario where a possible X-ray shell is unseen because it has become too cold to be detected through the intervening ISM (Smith et al 1985;Jones et al 1993).…”

Section: The Supernova Remnant W44mentioning

confidence: 97%

APEX observations of supernova remnants

Anderl

Güsten

2014

A&A

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Context. When supernova blast waves interact with nearby molecular clouds, they send slower shocks into these clouds. The resulting interaction regions provide excellent environments for the use of MHD shock models to constrain the physical and chemical conditions in these regions. Aims. The interaction of supernova remnants (SNRs) with molecular clouds gives rise to strong molecular emission in the far-IR and sub-mm wavelength regimes. The application of MHD shock models in the interpretation of this line emission can yield valuable information on the energetic and chemical impact of SNRs. Methods. New mapping observations with the APEX telescope in 12 CO (3-2), (4-3), (6-5), (7-6), and 13 CO (3-2) towards two regions in the SNR W44 are presented. Integrated intensities are extracted on five different positions, corresponding to local maxima of CO emission. The integrated intensities are compared to the outputs of a grid of models, which combine an MHD shock code with a radiative transfer module based on the large velocity gradient approximation. Results. All extracted spectra show ambient and line-of-sight components as well as blue-and red-shifted wings indicating the presence of shocked gas. Basing the shock model fits only on the highest-lying transitions that unambiguously trace the shock-heated gas, we find that the observed CO line emission is compatible with non-stationary shocks and a pre-shock density of 10 4 cm −3 . The ages of the modelled shocks scatter between values of ∼1000 and ∼3000 years. The shock velocities in W44F are found to lie between 20 km s −1 and 25 km s −1 , while in W44E fast shocks (30-35 km s −1 ) as well as slower shocks (∼20 km s −1 ) are compatible with the observed spectral line energy diagrams. The pre-shock magnetic field strength components perpendicular to the line of sight in both regions have values between 100 µG and 200 µG. Our best-fitting models allow us to predict the full ladder of CO transitions, the shocked gas mass in one beam as well as the momentum and energy injection.

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Galactic Supernova Remnants

Aschenbach

1985

X-Ray Astronomy in the Exosat Era

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Einstein Observations of the SNRs IC443, W44 and W49B

Cited by 4 publications

References 12 publications

An observation of IC 443 in the forbidden coronal lambda 6374 line

An observation of IC 443 in the forbidden coronal lambda 6374 line

APEX observations of supernova remnants

Galactic Supernova Remnants

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